标题： TESS观测的全食接触双星的基本参数 显示英文标题

标题： Fundamental Parameters for Totally Eclipsing Contact Binaries Observed by TESS

摘要： 通过光度方法单独确定质量比，完全食双星提供了一个独特的机会，消除了对光谱数据的需求。 研究低质量比（LMR）的接触双星对于推进我们对双星演化和罕见光学瞬变现象——称为红新星的形成理解至关重要。 我们从凌日系外行星勘测卫星中识别出143个完全食接触双星。 这些高精度的光曲线揭示了一个明显的奥康奈尔效应，我们通过在主星上引入一个冷斑来解释这一现象。 训练一个包含冷斑参数的神经网络模型，可以比Phoebe快两个数量级生成高精度的光曲线。 利用神经网络（NNnol3）模型结合马尔可夫链蒙特卡洛算法，我们迅速得出了这些系统的基本参数。 通过利用轨道周期与半长轴之间的关系，使用随机抽样一致性算法，我们估计了它们的绝对参数。 我们的分析识别出96个质量比低于0.25的目标，这些目标在任何之前的目录中都没有列出，因此标志着新的LMR系统候选者的发现。 假设所有143个双星系统在参数估计过程中受到第三光的影响，我们训练了一个考虑第三光的神经网络（NNl3）模型。 然后我们计算了质量比ql3（考虑第三光）与qnol3（忽略第三光）之间的残差。 对于这些残差，第25百分位数（Q1）为0.012，中位数（Q2）为0.026，第75百分位数（Q3）为0.05。 显示英文摘要

摘要： Totally eclipsing contact binaries provide a unique opportunity to accurately determine mass ratios through photometric methods alone, eliminating the need for spectroscopic data. Studying low mass ratio (LMR) contact binaries is crucial for advancing our understanding of binary star evolution and the formation of rare optical transients known as red novae. We identified 143 totally eclipsing contact binaries from the Transiting Exoplanet Survey Satellite. These high-precision light curves reveal a distinct O'Connell effect, which we interpret by introducing a cool spot on the primary star. Training a neural network model that includes cool spot parameters can generate a high-precision light curve 2 orders of magnitude faster than Phoebe. Utilizing the neural network (NNnol3) model combined with the Markov Chain Monte Carlo algorithm, we rapidly derived the fundamental parameters of these systems. By leveraging the relationship between orbital period and semimajor axis using the Random Sample Consensus algorithm, we estimated their absolute parameters. Our analysis identified 96 targets with mass ratios below 0.25, all of which were not listed in any previous catalog, thus signifying the discovery of new LMR system candidates. Assuming all 143 binary systems are affected by a third light during parameter estimation, we train a neural network (NNl3) model considering the third light. Then we calculate the residuals between the mass ratio ql3 (considering the third light) and qnol3 (neglecting it). For these residuals, the 25th percentile (Q1) is 0.012, the median (Q2) is 0.026, and the 75th percentile (Q3) is 0.05.